Many processes at work in low-mass (\(M_*\le 2\)  M\(_\) ) young stars influence their formation and evolution. Two of the most important ones are accretion and ejection of material onto and emanating from young stars, such as T Tauri stars (TTSs). These TTS are low-mass pre-main sequence stars which are commonly divided into two main classes: classical T Tauri stars (CTTSs), which are younger (\(\sim \) 10\(^6\)  yr) and more actively accreting than weak-line T Tauri stars (WTTS), which are often older (\(\sim \) 10\(^7\)  yr) and at the end of the accretion phase [1]}, [2]}, [3]}. The CTTSs demonstrate a rich emission spectrum mostly due to accretion of material theorised to be structured as funnels, flowing along the stellar magnetic field lines from the inner disk to the stellar surface [3]}. Other spectral lines come from the ejection phenomena. They are varied in their structures (e.g. jets and winds) and velocities, depending on the conditions from which they originate; however, it has been shown that a strong link between ejection and accretion exists [5]}.
